In Sec.  we have discussed a particular choice of the tapering frequency (\(f^{\text{tape}}_{22} = 0.35f_{22}^{\rm {peak}}\) ). Historically, this choice was motivated by comparisons of the FTI results with TIGER results In the LIGO-Virgo analyses [1]}, [2]}, [3]}, [4]}, [5]}, the TIGER code [6]} used the \(\tt {IMRPhenomD}\)  waveform model where the transition frequency between the inspiral and intermediate regions occurs close to \(f^{\text{tape}}_{22} = 0.35f_{22}^{\rm {peak}}\) .. Nevertheless, given that the FTI
method allows for flexibility in the tapering frequency, unlike
TIGER, we want to understand the effects of varying it. It is
also theoretically difficult to justify exactly where (i.e., at
which orbital frequency) the inspiral ends. We thus allow the
tapering frequency to vary up until the (approximate) merger
frequency, \(f_{22}^{\mathrm {peak}}\) , and explore its impact on our
results. Varying the tapering frequency beyond the merger frequency
would not make much sense for an inspiral test. We note that FTI analysis of
BNS would not be affected by increasing the default tapering frequency, because for such
systems, higher tapering frequency lie outside the sensitivity bandwidth of current
GW detectors (e.g., \(0.35 f_{22}^{\rm {peak}} \simeq 1350\)  Hz for GW170817).
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